Several studies have been showing that cosmic ray intensity variations observed at the Earth surface can be a useful tool to analyze and predict space weather and climate phenomena. However, before reach the ground level, the cosmic ray particles interact with different atmospheric atoms. This results in the generation of different secondary particles that are differently affected by atmospheric effects. For example, data from neutron monitors, which are widely used to study cosmic ray flux changes related to space phenomena, are significantly affected by atmospheric pressure changes. Thus, for a more detailed study of these instruments’ data, it is necessary to know very well how works the pressure affects secondary neutrons. In this way, we seek to understand how this effect changes according to the cosmic rays’ energy. Thus, in this work, we compare how the barometric coefficient ($\beta$), which quantifies the pressure effect on the cosmic ray intensity, changes with the geomagnetic cutoff rigidity ($R_C$), which quantifies the minimal rigidity/energy that a primary particle needs to reach a given location in a chosen direction. To do that, we used data recorded between January 2008 to December 2016 by several neutron monitors around the globe with $R_C$ from 0.1 to 8.3 GV. We experimentally obtained $\beta$ in two ways: (I) the typical one, which does not explicitly consider isotropic variations unrelated to the pressure effect; and (II) one that considers such variations by using coupling coefficients and a reference neutron monitor station. Like other works, we found that the pressure effect seems to present a logarithmic relation with the cutoff rigidity when we estimate $\beta$ through the typical method used. On the other hand, we found that the pressure effect linearly decreases with the cutoff rigidity when considering an adjustment in this typical method to eliminate external isotropic variations. This linear relation appears to not change accordingly to the reference monitor chosen. These results enhance our knowledge of how the pressure effect globally acts on the cosmic ray intensity observed at ground level and, consequently, improves future analysis about global changes in the cosmic ray flux related to space weather phenomena.

多项研究表明，在地球表面观测到的宇宙射线强度变化可以成为分析和预测空间天气和气候现象的有用工具。然而，在到达地面之前，宇宙射线粒子与不同的大气原子相互作用。这导致产生不同的次级粒子，这些粒子受大气效应的影响不同。例如，广泛用于研究与空间现象相关的宇宙射线通量变化的中子监测器的数据受到大气压力变化的显着影响。因此，为了更详细地研究这些仪器的数据，有必要非常了解压力如何影响二次中子。通过这种方式，我们试图了解这种效应是如何根据宇宙射线的能量而变化的。因此，在这项工作中，$\beta$)，量化压力对宇宙射线强度的影响，随地磁截止刚度 (${\mathrm{电阻}}_C$)，它量化了初级粒子在选定方向上到达给定位置所需的最小刚度/能量。为此，我们使用了全球多个中子监测器在 2008 年 1 月至 2016 年 12 月期间记录的数据，其中包括${\mathrm{电阻}}_C$从 0.1 到 8.3 GV。我们通过实验得到$\beta$两种方式：（I）典型的一种，没有明确考虑与压力效应无关的各向同性变化；(II) 通过使用耦合系数和参考中子监测站来考虑这种变化。与其他作品一样，我们发现，当我们估计时，压力效应似乎与截止刚度呈对数关系$\beta$通过使用的典型方法。另一方面，我们发现当考虑在这种典型方法中进行调整以消除外部各向同性变化时，压力效应随截止刚度线性降低。这种线性关系似乎不会随着所选的参考监视器而改变。这些结果增强了我们对全球压力效应如何影响在地面观测到的宇宙射线强度的认识，从而改进了未来对与空间天气现象相关的宇宙射线通量全球变化的分析。